The metallicity of galaxies and its evolution with redshift is of paramount importance for understanding galaxy formation. It is important to directly probe the metal abundances in the neutral gas in star-forming galaxies (SFGs) , where the bulk of the metals may be contained. This can be done using absorption lines in the Far UV. We have developed techniques to do this in SFGs using FUSE data, where the absorption is measured for sightlines toward bright SF regions within the galaxy itself. FUSE results suggest that in I Zw 18 that abundances in the neutral gas may be up to 0.5 dex lower than in the ionized gas. The advent of COS on HST now allows a significant advances over FUSE. We are obtaining absorption line spectroscopy with G130M (~1150-1450A) in the same sample for which we already have crude constraints from FUSE. The results will provide important new insights into the metallicities of galaxies, and into outstanding problems at high redshift such as the observed offset between the metallicities of Lyman Break Galaxies and Damped Lyman Alpha systems. Here we present the preliminary results of a few galaxies, including the renowned low-metallicity blue compact dwarf galaxies SBS1415+437, NGC5253 and the super-solar metallicity SFG M83.